If you have determined the parallactic displacement f of Venus on the sun's disc by combining two photos which have been taken simultaneously from different sites you can derive the distance to the sun or, respectively, the sun's parallax π_{S} with the following equation (see the related paper (in German or in English)):
In order to get an own measure for the Astronomical Unit you need to determine, among other quantities, the radius r_{V} of Venus' orbit or, to be more precise, the relation r_{V} /r_{E} between the radii of the orbits of Venus and the Earth.
Therefore, in this project we propose methods of determining the radius of Venus' orbit by an own measurement.
1. The maximum angular distance between the sun and Venus |
a. Direct measurement |
b. Measuring the equatorial positions of Venus and the Sun |
2. Observing Venus during her retrograde motion |
a. Special case |
b. Example 1 |
c. Generalisation |
d. Example 2 |
3. Former Results |
There are several possibilities for this measurement:
All of these methods make use of the following simplifications:
When the angular distance between Sun and Venus, observed from Earth, has its maximum value the triangle Sun - Venus - Earth is rectangular.
Therefore, the radius of Venus' orbit, in Astronomical Units, can easily be determined by measuring the maximum angular distance between Sun and Venus:
Because Venus will reach the maximum angular distance to the Sun around the
end of March 2012 (to be precise: March, 27^{th}) the suitable time for doing these measurements are
the weeks of March and April 2012! In these weeks, Venus will play the role of
the evening star so that the measurements can be done in the evening.
The following possibility will occur after the transit in August 2012 (August, 15^{th}). Then, Venus will act as the morning star.
The simplest method to measure the angle and to determine its maximum is to observe both objects above the horizont, simultaneously. If you observe Venus at the night sky early in the evening you will be able to find her shortly before sunset on the following days.
Proposals for rough measurements of the angle: (You may get an impression of the measurements on our first result page build for the transit in 2004)
This method is more precise than that described above. But it is more indirect and you need more knowledge (about celestial coordinates and sideral time, for instance) and more mathematical abilities (transformation of coordinates and so on).
The simplest method of measuring the equatorial position (α_{sun},δ_{sun}) of the Sun is to measure the exact time of its culmination and its maximum elevation. Then, there holds a simple relation between declination of the Sun, geographical latitude of the observer and the maximum elevation, for instance with a gnomon (see also geographical coordinates):
(for northern latitude)
(for southern latitude)
The right ascension of the sun is just the exact local sideral time of the time of culmination.
The easiest method of determining the celestial position of Venus is to observe her exact position among the stars after sunset (or before sunrise) and draw her into a sky map from which you can read the equatorial coordinates.
Moon, Venus and Mars in the evening of March, 27th, 2012
For this method, you have to measure the azimuth A, for instance with a magnetic compass, and the elevation h above the horizont and the exact time of your measurement. From these values, you can derive the equatorial coordinates by the following algorithm:
From the hour angle τ, you can derive the right ascension when you know the local sideral time:
If you know the equatorial positions of Venus and the sun it is not difficult to calculate their angular distance by the following formular (see below):
This method can be applied only in a short time interval around the transit, that is between May 15th, 2012 and June 27th, 2012!
Venus' retrograde motion between May, 15th, and June, 27th, 2012
Around the inferior conjunction of Venus, at the sky the planet will move retrogradely that means opposite to its usual direction (from east to west). That's why Venus overtakes the earth in that time. The picture below gives an explanation for this fact not only in a qualitative way but in a quantitative, too.
Explanation of the retrograde motion of a superior planet. In the case of the inferior planet Venus you must change the letters P and E. The argumentation remains unaltered.
In the triangle sun - E_{1} - P_{1}, the following equation holds:
Looking at the triangle sun - E_{1} - S you may realize the following identity:
Combining the both equations, we get the following result:
We hope that we will be able to observe and to measure Venus's position in its inferior conjunction, that is during its transit! Thus, we can measure its right ascension and declination on that day (see geographical position). If we will be able to measure Venus' position on an additional day during its retrograde motion we can determine the anglular distance η between these both positions by the following relation:
The central angles at the Sun can be derived from the mean daily motion of the planets which are due to their sideral periods:
In 2004, we offered an example for this calculation. It may serve as an illustration, here.
If we will be unlucky and not able to observe the transit we, nevertheless, can apply the above method by measuring Venus' position during its retrograde motion twice. In this case, the following equation must hold:
In this equation, the single angles η_{1} and η_{2} are unknown. Only the angle η=η_{2}-η_{1} has been measured. The central angles are again determined with respect to the date of conjunction.
The following function f must, therefore, be zero at the point η_{1}:
This is a well known numerical problem and can be solved by trial and error, by a graphical method or by a numerical algorithm, respectively. You may download a little program which does the work for you.
In 2004, we offered an example for this generalized method, too.
For our 2004 project, groups of students in Fürstenwalde und Essen, Germany, have determined the radius of Venus' orbit between the end of December 2002 and the end of January 2003. The results are shortly combined in a result page of our 2004 project.
The mean value of these measurements is:
Editors: | Udo Backhaus |
last update: 01.04.2012 | |||
Stephan Breil |